Details
| Original language | English |
|---|---|
| Article number | L24 |
| Number of pages | 30 |
| Journal | Astrophysical Journal Letters |
| Volume | 882 |
| Issue number | 2 |
| Publication status | Published - 9 Sept 2019 |
Abstract
We present results on the mass, spin, and redshift distributions with phenomenological population models using the 10 binary black hole (BBH) mergers detected in the first and second observing runs completed by Advanced LIGO and Advanced Virgo. We constrain properties of the BBH mass spectrum using models with a range of parameterizations of the BBH mass and spin distributions. We find that the mass distribution of the more massive BH in such binaries is well approximated by models with no more than 1% of BHs more massive than 45 M and a power-law index of (90% credibility). We also show that BBHs are unlikely to be composed of BHs with large spins aligned to the orbital angular momentum. Modeling the evolution of the BBH merger rate with redshift, we show that it is flat or increasing with redshift with 93% probability. Marginalizing over uncertainties in the BBH population, we find robust estimates of the BBH merger rate density of R= (90% credibility). As the BBH catalog grows in future observing runs, we expect that uncertainties in the population model parameters will shrink, potentially providing insights into the formation of BHs via supernovae, binary interactions of massive stars, stellar cluster dynamics, and the formation history of BHs across cosmic time.
Keywords
- black holes, gravitational waves, statistical
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Astronomy and Astrophysics
- Earth and Planetary Sciences(all)
- Space and Planetary Science
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In: Astrophysical Journal Letters, Vol. 882, No. 2, L24, 09.09.2019.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo
AU - The LIGO Scientific Collaboration
AU - The Virgo Collaboration
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Abraham, S.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Allen, G.
AU - Allocca, A.
AU - Aloy, M. A.
AU - Altin, P. A.
AU - Amato, A.
AU - Ananyeva, A.
AU - Anderson, S. B.
AU - Anderson, W. G.
AU - Angelova, S. V.
AU - Antier, S.
AU - Appert, S.
AU - Arai, K.
AU - Araya, M. C.
AU - Areeda, J. S.
AU - Arène, M.
AU - Arnaud, N.
AU - Arun, K. G.
AU - Ascenzi, S.
AU - Ashton, G.
AU - Aston, S. M.
AU - Astone, P.
AU - Aubin, F.
AU - Danilishin, S. L.
AU - Danzmann, K.
AU - Heurs, M.
AU - Hreibi, A.
AU - Lück, H.
AU - Steinmeyer, D.
AU - Vahlbruch, H.
AU - Wei, L.-w.
AU - Wilken, D. M.
AU - Willke, B.
AU - Wittel, H.
AU - Bose, Sukanta
AU - Brown, D. D.
AU - Chen, Y. B.
AU - Hanke, Manuela
AU - Hennig, J.
AU - Kumar, Sanjeev
AU - Lang, R. N.
AU - Lee, H. K.
AU - Lee, H. M.
AU - Lee, H. W.
AU - Lee, J.
AU - Li, X.
AU - Sanders, J. R.
AU - Schmidt, Patricia
AU - Sun, L.
AU - Wang, Y. F.
AU - Wu, D. S.
AU - Zhang, L.
AU - Zhu, X. J.
AU - Zhou, Minchuan
AU - Bergmann, Gerald
AU - Bisht, Aparna
AU - Bode, Nina
AU - Booker, P.
AU - Brinkmann, Marc
AU - Cabero, M.
AU - de Varona, O.
AU - Hochheim, S.
AU - Dent, T.
AU - Doravari, S.
AU - Junker, J.
AU - Kaufer, Stefan
AU - Kirchhoff, R.
AU - Koch, Patrick
AU - Koper, N.
AU - Köhlenbeck, S. M.
AU - Kringel, Volker
AU - Karvinen, Kai S.
AU - Khan, S.
AU - Leavey, S.
AU - Lehmann, J.
AU - Lough, James
AU - Mehmet, Moritz
AU - Mukherjee, Arunava
AU - Mukund, Nikhil
AU - Nery, M.
AU - Ohme, F.
AU - Oppermann, P.
AU - Rüdiger, A.
AU - Phelps, M.
AU - Puncken, O.
AU - Schreiber, Emil
AU - Schulte, B. W.
AU - Setyawati, Y.
AU - Steinke, M.
AU - Standke, M.
AU - Thies, Fabian
AU - Weinert, Michael
AU - Wellmann, F.
AU - Weßels, Peter
AU - Wimmer, Maximilian H.
AU - Winkler, W.
AU - Woehler, J.
N1 - Funding Information: Supported by an MRC/PMAC Fellowship, MRC Canada, Alberta Heritage Foundation of Medical Research (AHFMR) and Glaxo-Heritage.
PY - 2019/9/9
Y1 - 2019/9/9
N2 - We present results on the mass, spin, and redshift distributions with phenomenological population models using the 10 binary black hole (BBH) mergers detected in the first and second observing runs completed by Advanced LIGO and Advanced Virgo. We constrain properties of the BBH mass spectrum using models with a range of parameterizations of the BBH mass and spin distributions. We find that the mass distribution of the more massive BH in such binaries is well approximated by models with no more than 1% of BHs more massive than 45 M and a power-law index of (90% credibility). We also show that BBHs are unlikely to be composed of BHs with large spins aligned to the orbital angular momentum. Modeling the evolution of the BBH merger rate with redshift, we show that it is flat or increasing with redshift with 93% probability. Marginalizing over uncertainties in the BBH population, we find robust estimates of the BBH merger rate density of R= (90% credibility). As the BBH catalog grows in future observing runs, we expect that uncertainties in the population model parameters will shrink, potentially providing insights into the formation of BHs via supernovae, binary interactions of massive stars, stellar cluster dynamics, and the formation history of BHs across cosmic time.
AB - We present results on the mass, spin, and redshift distributions with phenomenological population models using the 10 binary black hole (BBH) mergers detected in the first and second observing runs completed by Advanced LIGO and Advanced Virgo. We constrain properties of the BBH mass spectrum using models with a range of parameterizations of the BBH mass and spin distributions. We find that the mass distribution of the more massive BH in such binaries is well approximated by models with no more than 1% of BHs more massive than 45 M and a power-law index of (90% credibility). We also show that BBHs are unlikely to be composed of BHs with large spins aligned to the orbital angular momentum. Modeling the evolution of the BBH merger rate with redshift, we show that it is flat or increasing with redshift with 93% probability. Marginalizing over uncertainties in the BBH population, we find robust estimates of the BBH merger rate density of R= (90% credibility). As the BBH catalog grows in future observing runs, we expect that uncertainties in the population model parameters will shrink, potentially providing insights into the formation of BHs via supernovae, binary interactions of massive stars, stellar cluster dynamics, and the formation history of BHs across cosmic time.
KW - black holes
KW - gravitational waves
KW - statistical
UR - http://www.scopus.com/inward/record.url?scp=85073031675&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/ab3800
DO - 10.3847/2041-8213/ab3800
M3 - Article
VL - 882
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 2
M1 - L24
ER -